There are suggestions that both the magnetic field and the coupling of the gas to the magnetic field could be strong enough for magnetospheric accretion to occur [1]}, [2]}. Applying the [3]} scaling to the luminosities of young planets, [4]} found that they should have a surface dipole field \(B\sim 0.5\) –1 kG. Using typical accretion rates [5]}, the resulting estimate of the magnetospheric (or Alfvén) radius is usually larger than the planet radius, which holds even more for forming planets, which might have an even higher luminosity [6]}. Taken together with the estimate of a relatively low magnetic diffusivity, this suggests that planets could indeed accrete magnetospherically [2]}, [8]}. Nevertheless, one should keep in mind
that the validity of the [3]} scaling for forming planets has yet to be shown, especially since they are not necessarily fully convective [10]}, [11]}.
Estimating whether planets can accrete magnetospherically might also depend on the field topology,
which for CTTSs has significant non-dipole components [12]}.
